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authorAaron LI <aly@aaronly.me>2017-06-23 10:41:47 +0800
committerAaron LI <aly@aaronly.me>2017-06-23 10:41:47 +0800
commit4de4dac9f909d6cbc7af1021eb403524983a436d (patch)
treef7a4be758ab4c5538eaa15374ed7d47a887caf78 /fg21sim/extragalactic
parenteb660ae70db40d36418f1e4eb886fd9bb02af1a7 (diff)
downloadfg21sim-4de4dac9f909d6cbc7af1021eb403524983a436d.tar.bz2
emission.py: Add power(), flux(), brightness() methods
Diffstat (limited to 'fg21sim/extragalactic')
-rw-r--r--fg21sim/extragalactic/clusters/emission.py136
1 files changed, 111 insertions, 25 deletions
diff --git a/fg21sim/extragalactic/clusters/emission.py b/fg21sim/extragalactic/clusters/emission.py
index 1374b52..345e3db 100644
--- a/fg21sim/extragalactic/clusters/emission.py
+++ b/fg21sim/extragalactic/clusters/emission.py
@@ -1,8 +1,15 @@
-# Copyright (c) 2017 Weitian LI <liweitianux@live.com>
+# Copyright (c) 2017 Weitian LI <weitian@aaronly.me>
# MIT license
"""
-Calculate the synchrotron emission for simulated radio halos.
+Calculate the synchrotron emission and inverse Compton emission
+for simulated radio halos.
+
+References
+----------
+[1] Cassano & Brunetti 2005, MNRAS, 357, 1313
+ http://adsabs.harvard.edu/abs/2005MNRAS.357.1313C
+ Appendix.C
"""
import logging
@@ -11,7 +18,11 @@ import numpy as np
import scipy.integrate
import scipy.special
-from ...utils.units import (Units as AU, Constants as AC)
+from ...utils.units import (Units as AU,
+ UnitConversions as AUC,
+ Constants as AC)
+from ...utils.convert import Fnu_to_Tb_fast
+from ...utils.cosmology import Cosmology
logger = logging.getLogger(__name__)
@@ -19,18 +30,34 @@ logger = logging.getLogger(__name__)
class SynchrotronEmission:
"""
- Calculate the synchrotron emission from a given population
+ Calculate the synchrotron emission spectrum from a given population
of electrons.
- References
+ Parameters
----------
- [1] Cassano & Brunetti 2005, MNRAS, 357, 1313
- http://adsabs.harvard.edu/abs/2005MNRAS.357.1313C
- Appendix.C
+ B : float
+ The assumed uniform magnetic field of the galaxy cluster.
+ Unit: [uG]
+ p : `~numpy.ndarray`
+ The momentum grid adopted when solving the Fokker-Planck equation.
+ Unit: [mec]
+ n_e : `~numpy.ndarray`
+ Electron spectrum by solving the Fokker-Planck equation.
+ Unit: [cm^-3 mec^-1]
+ radius, float
+ The radius of the galaxy cluster/halo, within which the uniform
+ magnetic field and electron distribution are assumed.
+ Unit: [kpc]
+ z : float
+ Redshift of the galaxy cluster/halo
"""
- def __init__(self, B):
- # Uniform magnetic field strength
+ def __init__(self, B, p, n_e, radius, z):
self.B = B # [uG]
+ self.p = p
+ self.n_e = n_e
+ self.z = z
+ self.radius = radius # [kpc]
+ self.cosmo = Cosmology()
@property
def frequency_larmor(self):
@@ -69,7 +96,8 @@ class SynchrotronEmission:
nu = (3/2) * p**2 * np.sin(theta) * nu_L
return nu
- def F(self, x):
+ @staticmethod
+ def F(x):
"""
Synchrotron kernel function.
"""
@@ -77,22 +105,16 @@ class SynchrotronEmission:
a=x, b=np.inf)[0]
return val
- def emissivity(self, nu, p, n_e):
+ def emissivity(self, nu):
"""
Calculate the synchrotron emissivity (power emitted per volume
- and per frequency) at the specified frequency from the given
- electron number & energy distribution
+ and per frequency) at the requested frequency.
Parameters
----------
nu : float
- Frequency (unit: MHz) where to calculate the emissivity.
- p : `~numpy.ndarray`
- The momentum grid adopted when solving the Fokker-Planck equation.
- Unit: [mec]
- n_e : `~numpy.ndarray`
- Electron spectrum by solving the Fokker-Planck equation.
- Unit: [cm^-3 mec^-1]
+ Frequency where to calculate the emissivity.
+ Unit: [MHz]
Returns
-------
@@ -106,12 +128,76 @@ class SynchrotronEmission:
return (np.sin(theta)**2 * _n_e * self.F(x))
coef = np.sqrt(3) * AC.e**3 * self.B / AC.c # multiplied a [mec]
- func_p = np.zeros(p.shape)
- for i in range(len(p)):
+ func_p = np.zeros(self.p.shape)
+ for i in range(len(self.p)):
# Integrate over ``theta``
func_p[i] = scipy.integrate.quad(
- lambda t: func(t, p[i], n_e[i]),
+ lambda t: func(t, self.p[i], self.n_e[i]),
a=0, b=np.pi/2)[0]
# Integrate over ``p``
- j_nu = coef * scipy.integrate.trapz(func_p, p)
+ j_nu = coef * scipy.integrate.trapz(func_p, self.p)
return j_nu
+
+ def power(self, nu):
+ """
+ Calculate the synchrotron power (power emitted per frequency)
+ at the requested frequency.
+
+ Returns
+ -------
+ P_nu : float
+ Synchrotron power at frequency ``nu``.
+ Unit: [erg/s/Hz]
+ """
+ r_cm = self.radius * AUC.kpc2cm
+ volume = (4.0/3.0) * np.pi * r_cm**3
+ P_nu = self.emissivity(nu) * volume
+ return P_nu
+
+ def flux(self, nu):
+ """
+ Calculate the synchrotron flux (power observed per frequency)
+ at the requested frequency.
+
+ Returns
+ -------
+ F_nu : float
+ Synchrotron flux at frequency ``nu``.
+ Unit: [Jy] = 1e-23 [erg/s/cm^2/Hz]
+ """
+ DL = self.cosmo.DL(self.z) * AUC.Mpc2cm # [cm]
+ P_nu = self.power(nu)
+ F_nu = 1e23 * P_nu / (4*np.pi * DL*DL) # [Jy]
+ return F_nu
+
+ def brightness(self, nu, pixelsize):
+ """
+ Calculate the synchrotron surface brightness (power observed
+ per frequency and per solid angle) at the specified frequency.
+
+ NOTE
+ ----
+ If the radio halo has solid angle less than the pixel area, then
+ it is assumed to have solid angle of 1 pixel.
+
+ Parameters
+ ----------
+ pixelsize : float
+ The pixel size of the output simulated sky image
+ Unit: [arcmin]
+
+ Returns
+ -------
+ Tb : float
+ Synchrotron surface brightness at frequency ``nu``.
+ Unit: [K] <-> [Jy/pixel]
+ """
+ DA = self.cosmo.DL(self.z) * AUC.Mpc2cm # [cm]
+ radius = self.radius * AUC.kpc2cm # [cm]
+ omega = (np.pi * radius**2 / DA**2) * AUC.rad2deg**2 # [deg^2]
+ pixelarea = (pixelsize/60.0) ** 2 # [deg^2]
+ if omega < pixelarea:
+ omega = pixelarea
+ F_nu = self.flux(nu)
+ Tb = Fnu_to_Tb_fast(F_nu, omega, nu)
+ return Tb